Development of a Monte Carlo code for the data analysis of the {sup 18}F(p,α){sup 15}O reaction at astrophysical energies
- Dipartimento di Fisica e Astronomia, Catania, Italy and INFN-Laboratori Nazionali del Sud, Catania (Italy)
- INFN-Laboratori Nazionali del Sud, Catania (Italy)
- Universitá di Enna KORE, Enna, Italy and INFN-Laboratori Nazionali del Sud, Catania (Italy)
- Riken, Wako, Tokyo, Japan and Center for Nuclear Study, The University of Tokyo (Japan)
- Center for Nuclear Study, The University of Tokyo (Japan)
- Department of Physics, Tohoku University, Sendai (Japan)
- Department of Physics, Yamagata University, Yamagata (Japan)
- Rare Isotope Science Project, Institute for Basic Science, Yuseong-daero, Yuseong-gu, Daejeon 305-811 (Korea, Republic of)
- Department of Physics, Kyushu University, Fukuoka (Japan)
- Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse, Orsay (France)
- Institut de Physique Nucléaire, IN2P3, Orsay (France)
Novae are astrophysical events (violent explosion) occurring in close binary systems consisting of a white dwarf and a main-sequence star or a star in a more advanced stage of evolution. They are called 'narrow systems' because the two components interact with each other: there is a process of mass exchange with resulting in the transfer of matter from the companion star to the white dwarf, leading to the formation of this last of the so-called accretion disk, rich mainly of hydrogen. Over time, more and more material accumulates until the pressure and the temperature reached are sufficient to trigger nuclear fusion reactions, rapidly converting a large part of the hydrogen into heavier elements. The products of 'hot hydrogen burning' are then placed in the interstellar medium as a result of violent explosions. Studies on the element abundances observed in these events can provide important information about the stages of evolution stellar. During the outbursts of novae some radioactive isotopes are synthesized: in particular, the decay of short-lived nuclei such as {sup 13}N and {sup 18}F with subsequent emission of gamma radiation energy below 511 keV. The gamma rays from products electron-positron annihilation of positrons emitted in the decay of {sup 18}F are the most abundant and the first observable as soon as the atmosphere of the nova starts to become transparent to gamma radiation. Hence the importance of the study of nuclear reactions that lead both to the formation and to the destruction of {sup 18}F. Among these, the {sup 18}F(p,α){sup 15}O reaction is one of the main channels of destruction. This reaction was then studied at energies of astrophysical interest. The experiment done at Riken, Japan, has as its objective the study of the {sup 18}F(p,α){sup 15}O reaction, using a beam of {sup 18}F produced at CRIB, to derive important information about the phenomenon of novae. In this paper we present the experimental technique and the Monte Carlo code developed to be used in the data analysis process.
- OSTI ID:
- 22390987
- Journal Information:
- AIP Conference Proceedings, Vol. 1645, Issue 1; Conference: Carpathian Summer School of Physics 2014, Sinaia (Romania), 13-26 Jul 2014; Other Information: (c) 2015 AIP Publishing LLC; Country of input: International Atomic Energy Agency (IAEA); ISSN 0094-243X
- Country of Publication:
- United States
- Language:
- English
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Related Subjects
ACCRETION DISKS
ASTROPHYSICS
DATA ANALYSIS
ELECTRON-POSITRON INTERACTIONS
ELEMENT ABUNDANCE
EMISSION
FLUORINE 18 TARGET
HEAVY ION FUSION REACTIONS
HYDROGEN
HYDROGEN BURNING
KEV RANGE
MAIN SEQUENCE STARS
MONTE CARLO METHOD
NITROGEN 13
NOVAE
OXYGEN 15
PROTON REACTIONS
THERMONUCLEAR REACTIONS
WHITE DWARF STARS